The Borexino detector at the Laboratori Nazionali del Gran Sasso

Alimonti, A.; Arpesella, C.; Back, H. O.; Balata, M.; Bartolomei, D.; Bellefon, A. de; Bellini, G.; Benziger, J.; Bévilacqua, A.; Bondi, D.; Bonetti, S.; Brigatti, A.; Caccianiga, B.; Cadonati, L.; Calaprice, F.; Carraro, C.; Ceccet, G.; Ceresto, R.; Chavarría, Á.; Chen, A.; Chepurnov, A.; Cubauu, A.; Czech, W.; D’Angelo, D.; Dalnoki‐Veress, F.; Bari, A. de; Haas, E. de; Derbin, A.; Deutsch, Martin; Credico, A. Di; Ldovico, A. Di; Pietro, G. Di; Eisenstein, R. A.; Elisei, Fausto; Etenko, A.; Feiltitsch, F. von; Fernholz, Robert; Fomenko, K.; Ford, R.; Franco, D.; Freudiger, B.; Gärtner, Matthias; Galbiati, C.; Gattig, F.; Gazzana, S.; Gehman, V. M.; Giammarchi, M.; Giugni, D.; Goeger-Neff, M.; Goldbrunner, T.; Golubchikov, A.; Goretti, A.; Grieb, C.; Hagner, C.; Hampel, W.; Harding, Eric; Hardy, S.; Hartmann, F.; Hentig, R. von; Hertich, T.; Heusser, G.; Hult, M.; Ianni, A.; Jaenner, K.; Joyce, M.; Kerret, H. de; Kidner, S.; Kiko, J.; Kirsten, T.; Kobychev, V.; Korga, G.; Korschnik, G.; Kozlov, Yu. V.; Kryne, D.; Marche, P. La; Lagomarsino, V.; Laubenstein, M.; Lendvai, C.; Leung, M.; Lewke, T.; Litvinovich, E.; Loer, B.; Loeser, D.; Lombardi, P.; Ludhová, L.; Machulin, I.; Malvezzi, S.; Manco, A.; Maneira, J.; Maneschg, W.; Manno, I.; Manuzio, D.; Manuzio, G.; Marchelli, M.; Martemiano, A.; Masetti, F.; Mazzucato, U.; McCarty, K.; McKinsey, D. N.; Meindl, Q.; Meroni, E.; Miramonti, L.; Misiaszek, M.; Montanari, D.; Monzani, M. E.; Muratova, V.; Musico, P.; Neder, H.; Nelson, A.; Niedermeier, L.; Nisi, S.; Oberauer, L.; Obolensky, M.; Orsini, M.; Ortica, F.; Pallavicini, M.; Papp, L.; Parmeggiano, S.; Parodi, Mauro; Pelliccia, N.; Perasso, L.; Pocar, A.; Raghavan, R. S.; Ranucci, G.; Rau, W.; Razeto, A.; Resconi, E.; Risso, P.; Romani, A.; Rountree, D.; Sabelnikov, A.; Saggese, Paolo; Saldhana, R.; Salvo, C.; Scardaoni, R.; Schimizzi, D.; Schönert, S.; Schubeck, K. H.; Shutt, T.; Siccardi, F.; Simgen, H.; Skorokhvatov, M.; Smirnov, O.; Sonnenschein, A.; Soricelli, F.; Sotnikov, A.; Sukhotin, S.; Sule, C.; Suvorov, Y.; Tarasenkov, V. G.; Tartaglia, R.; Testera, G.; Vignaud, D.; Vital, S.; Vogelaar, R. B.; Vyrodov, V.; William, B.; Wójcik, Marcin; Wordel, R.; Wurm, M.; Zaimidoroga, O.; Zavatarelli, S.; Zuzel, G.

doi:10.1016/j.nima.2008.11.076

Cited by 375 publications

(312 citation statements)

References 40 publications

Supporting

Mentioning

308

Contrasting

Unclassified

Order By: Relevance

“…We refer to the LSV and WCV detectors together as the veto system of DarkSide-50. The DarkSide-50 detectors are located in Hall C of LNGS, in close proximity to and sharing many facilities with the Borexino experiment [6,7].…”

Section: Darkside-50 and Its Neutron Vetomentioning

confidence: 99%

Results from the first use of low radioactivity argon in a dark matter search

Agnes¹,

Agostino²,

Albuquerque³

et al. 2016

Phys. Rev. D

Self Cite

174

239

View full text Add to dashboard Cite

A b s tra c t: Nuclear recoil events produced by neutron scatters form one of the most important classes of background in WIMP direct detection experiments, as they may produce nuclear recoils that look exactly like W IMP interactions. In DarkSide-50, we both actively suppress and measure the rate of neutron-induced background events using our neutron veto, composed of a boron-loaded liquid scintillator detector within a water Cherenkov detector. This paper is devoted to the description of the neutron veto system of DarkSide-50, including the detector structure, the fundamentals of event reconstruction and data analysis, and basic performance parameters.

show abstract

Section: Darkside-50 and Its Neutron Vetomentioning

confidence: 99%

Results from the first use of low radioactivity argon in a dark matter search

Agnes¹,

Agostino²,

Albuquerque³

et al. 2016

Phys. Rev. D

Self Cite

174

239

View full text Add to dashboard Cite

show abstract

“…SNEWS has been set up to broadcast a reliable alert to the astronomy community when a supernova has been detected by several neutrino detectors within seconds of each other. Currently, Super-Kamiokande (Fukuda et al 2002;Ikeda et al 2007), LVD (Aglietta et al 2002), Borexino (Alimonti et al 2009) and IceCube (Ahrens et al 2004) contribute to SNEWS, with a number of other neutrino and gravitational wave detectors planning to join in the near future.…”

Section: Introductionmentioning

confidence: 99%

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

Self Cite

133

View full text Add to dashboard Cite

This paper describes the response of the IceCube neutrino telescope located at the geographic south pole to outbursts of MeV neutrinos from the core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a volume of ∼1 km 3 in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect large numbers of MeV neutrinos by observing a collective rise in all photomultiplier rates on top of the dark noise. With 2 ms timing resolution, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova at the galactic center, its sensitivity matches that of a background-free megaton-scale supernova search experiment. The sensitivity decreases to 20 standard deviations at the galactic edge (30 kpc) and 6 standard deviations at the Large Magellanic Cloud (50 kpc). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to A109, page 1 of 18 detect the neutronization burst, a short outbreak of ν e 's released by electron capture on protons soon after collapse. Tantalizing signatures, such as the formation of a quark star or a black hole as well as the characteristics of shock waves, are investigated to illustrate IceCube's capability for supernova detection.

show abstract

“…This type of experiments might be the most viable and successful in detecting type Ia supernovae, especially if a proton elastic scattering (PES) method is used (Beacom et al 2002). One example of such a device is the Borexino detector (Alimonti et al 2009). Although it is perhaps too small for detecting a thermonuclear supernova at a kpc distance, Borexino will be an essential testbed for the proposed and much larger LENA (Autiero et al 2007;Marrodán-Undagoitia et al 2006;Oberauer et al 2005) and other similar experiments (Maricic & the Hanohano collaboration 2010).…”

Section: Discussionmentioning

confidence: 99%

Probing thermonuclear supernova explosions with neutrinos

Odrzywołek¹,

Plewa²

2011

A&A

View full text Add to dashboard Cite

Aims. We present neutrino light curves and energy spectra for two representative type Ia supernova explosion models: a pure deflagration and a delayed detonation. Methods. We calculate the neutrino flux from β processes using nuclear statistical equilibrium abundances convoluted with approximate neutrino spectra of the individual nuclei and the thermal neutrino spectrum (pair+plasma). Results. Although the two considered thermonuclear supernova explosion scenarios are expected to produce almost identical electromagnetic output, their neutrino signatures appear vastly different, which allows an unambiguous identification of the explosion mechanism: a pure deflagration produces a single peak in the neutrino light curve, while the addition of the second maximum characterizes a delayed-detonation. We identified the following main contributors to the neutrino signal: (1) weak electron neutrino emission from electron captures (in particular on the protons 55 Co and 56 Ni) and numerous β-active nuclei produced by the thermonuclear flame and/or detonation front, (2) electron antineutrinos from positron captures on neutrons, and (3) the thermal emission from pair annihilation. We estimate that a pure deflagration supernova explosion at a distance of 1 kpc would trigger about 14 events in the future 50 kt liquid scintillator detector and some 19 events in a 0.5 Mt water Cherenkov-type detector. Conclusions. While in contrast to core-collapse supernovae neutrinos carry only a very small fraction of the energy produced in the thermonuclear supernova explosion, the SN Ia neutrino signal provides information that allows us to unambiguously distinguish between different possible explosion scenarios. These studies will become feasible with the next generation of proposed neutrino observatories.

show abstract

The Borexino detector at the Laboratori Nazionali del Gran Sasso

Cited by 375 publications

References 40 publications

Results from the first use of low radioactivity argon in a dark matter search

Results from the first use of low radioactivity argon in a dark matter search

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Probing thermonuclear supernova explosions with neutrinos

Contact Info

Product

Resources

About